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The Rossiter-McLaughlin (RM) effect is the radial velocity signal generatedwhen an object transits a rotating star. Stars rotate differentially and thisaffects the shape and amplitude of this signal, on a level that can no longerbe ignored with precise spectrographs. Highly misaligned planets provide aunique opportunity to probe stellar differential rotation via the RM effect, asthey cross several stellar latitudes. In this sense, WASP-7, and its hotJupiter with a projected misalignment of \sim 90{\deg}, is one of the mostpromising targets. The aim of this work is to understand if the stellardifferential rotation is measurable through the RM signal for systems with ageometry similar to WASP-7. In this sense, we use a modified version of SOAP3.0to explore the main hurdles that prevented the precise determination of thedifferential rotation of WASP-7. We also investigate whether the adoption ofthe next generation spectrographs, like ESPRESSO, would solve these issues.Additionally, we assess how instrumental and stellar noise influence thiseffect and the derived geometry of the system. We found that, for WASP-7, thewhite noise represents an important hurdle in the detection of the stellardifferential rotation, and that a precision of at least 2m/s or better isessential.

Can we detect the stellar differential rotation of WASP-7 through theRossiter-McLaughlin observations?